In this example, we wish to perform a short wavelength CVF scan of a
comet, reaching a S/N greater than 3 for a surface brightness of
2 mJy/''
. Here the background is estimated from the zodiacal
light model at the ecliptic pole, scaled by a factor of 5.
We will not use the full sampling of the CVF but instead
perform an integration every two positions. Thus the parameters for
this observation are the wavelength interval, here from 2.6 to
5.2 
m, and the increment, in units of CVF steps, between each
filter position, 2. We used the 6'' lens, and after a small number of
trials, selected an integration time of 6 s.
The results of this computation are shown on figure 
.
Here the upper curve refers to the S/N achieved at 5.2 m, and the
lower one to the S/N at 2.6 m. One sees that our observation can
reasonably be done in 
4000 s (plus 180 s for pointing).